Results 11 to 20 of about 1,207,200 (332)
Influence of grain size and composition on the contraction rates of planetary envelopes and on planetary migration [PDF]
Astronomy & Astrophysics, 2021 A crucial phase during planetary growth is the migration, when the planetary core has been assembled but has not yet opened a deep gap. During this phase, the planet is subject to fast type-I migration, which is mostly directed inwards, and the planet ...
B. Bitsch, S. Savvidou
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PLANETARY MIGRATION IN EVOLVING PLANETESIMAL DISKS [PDF]
International Journal of Modern Physics D, 2003 In the current paper, we further improved the model for the migration of planets introduced and extended to time-dependent planetesimal accretion disks by Del Popolo. In the current study, the assumption of Del Popolo, that the surface density in planetesimals is proportional to that of gas, is relaxed. In order to obtain the evolution of planetesimal
I. S. Yeşilyurt +2 more
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Planetary migration to large radii [PDF]
Monthly Notices of the Royal Astronomical Society, 2007 Accepted for publication in ...
Rebecca G. Martin +3 more
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Effect of wind-driven accretion on planetary migration [PDF]
Astronomy & Astrophysics, 2019 Context. Planetary migration is a key link between planet formation models and observed exoplanet statistics. So far, the theory of planetary migration has focused on the interaction of one or more planets with an inviscid or viscously evolving gaseous ...
C. Kimmig, C. Dullemond, W. Kley
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How planetary growth outperforms migration [PDF]
Astronomy & Astrophysics, 2018 Planetary migration is a major challenge for planet-formation theories. The speed of type-I migration is proportional to the mass of a protoplanet, while the final decade of growth of a pebble-accreting planetary core takes place at a rate that scales ...
A. Johansen, S. Ida, R. Brasser
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Is planetary migration inevitable?
, 2003 According to current theories, tidal interactions between a disk and an embedded planet may lead to the rapid migration of the protoplanet on a timescale shorter than the disk lifetime or estimated planetary formation timescales. Therefore, planets can form only if there is a mechanism to hold at least some of the cores back on their way in.
Caroline Terquem
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Planetary Migration in Protoplanetary Disks. [PDF]
, 2018 The known exoplanet population displays a great diversity of orbital architectures, and explaining the origin of this is a major challenge for planet formation theories.
R. Nelson
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Stopping inward planetary migration by a toroidal magnetic field [PDF]
Monthly Notices of the Royal Astronomical Society, 2003 We calculate the linear torque exerted by a planet on a circular orbit on a disc containing a toroidal magnetic field. All fluid perturbations are singular at the so--called magnetic resonances, where the Doppler shifted frequency of the perturbation matches that of a slow MHD wave propagating along the field line.
Caroline Terquem
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Planetary migration in gaseous protoplanetary disks [PDF]
Proceedings of the International Astronomical Union, 2007 AbstractTides come from the fact that different parts of a system do not fall in exactly the same way in a non-uniform gravity field. In the case of a protoplanetary disk perturbed by an orbiting, prograde protoplanet, the protoplanet tides raise a wake in the disk which causes the orbital elements of the planet to change over time.
F. Masset
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Preventing extinction in an age of species migration and planetary change
Conservation Biology, 2023 International and national conservation policies almost exclusively focus on conserving species in their historic native ranges, thus excluding species that have dispersed on their own accord or have been introduced by people.
Erick J. Lundgren +5 more
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